The peak frequency of GW spectrum produced from the EWPT is red-shifted to around the milli-Hertz band, which
falls right within the range of future space-based GW interferometers. The planned space-based GW experiments considered in this
work include the LISA [1]} interferometer as well as the proposed successors B-DECIGO [2]},
DECIGO [3]}, and BBO [4]}. For the auto-correlated experiments LISA and B-DECIGO, \(\mathcal {N}=1\) , while \(\mathcal {N}=2\)  for the cross-correlated experiments DECIGO and BBO.
Following Ref. [5]}, we assume a mission duration of \(\mathcal {T}_{\rm obs}=4\)  years
for all of the experiments. The SNR threshold value \(\rho _{\rm thr}\) , above which the GW signal is detectable for the experiment, and the other detector parameters are summarized in table REF . The experimental sensitivities are summarized in appendix .
<TABLE><FIGURE>